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Lys van grootste sterre

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Hierdie lys van grootste sterre is gerangskik volgens hul radius. Die meeteenheid is ’n sonradius (sowat 695 500 km). Sterre met 'n radius van tot 1 000 sonradiusse word aangedui, met 'n paar ander ter vergelyking.

Relatiewe groottes van die planete van die Sonnestelsel en verskeie bekende sterre, onder meer van die grootstes bekend: VY Canis Majoris, NML Cygni en UY Scuti.
  1. Mercurius < Mars < Venus < Aarde
  2. Aarde < Neptunus < Uranus < Saturnus < Jupiter
  3. Jupiter < Proxima Centauri < Son < Sirius
  4. Sirius < Pollux < Arcturus < Aldebaran
  5. Aldebaran < Rigel < Antares < Betelgeuse
  6. Betelgeuse < VY Canis Majoris < NML Cygni < UY Scuti

Die presiese volgorde van die sterre is nie honderd persent vasgestel nie:

  • Daar is taamlike onsekerhede oor geraamde waardes en groottes;
  • Die afstand na die verskillende sterre is nie oral ewe seker nie en dit beïnvloed die meting van die groottes;
  • Sommige sterre het ’n uitgebreide atmosfeer, is omring deur stof of pulseer, sodat hul radius nie presies bereken kan word nie;
  • Verskeie ander faktore kan ook die meting van die groottes beïnvloed.

Op dié lys is verskeie voorbeelde van sterre in uiters verre sterrestelsels, wat effens verskillende eienskappe het as die huidige grootste bekende sterre in die Melkweg. Sommige rooisuperreuse in die Magellaanse Wolke het byvoorbeeld na verwagting effens ander beperkende temperature en ligsterktes. Sulke sterre kan perke oorskry deur oor slegs ’n paar maande (of jaar) groot ontploffings of ’n verandering in hulle spektraaltipe te ondergaan.[1]

Die grootste ster wat waarskynlik nog ontdek is, is Stephenson 2-18. As dit in die plek van die Son geplaas word, sal dit tot anderkant Saturnus se wentelbaan strek.

Lys

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Grootste sterre in die Melkweg
Sternaam Sonradius
(Son = 1) 		Notas Verwysings
Stephenson 2-18 2 150 Geleë naby die massiewe oop sterreswerm Stephenson 2, waar 26 rooisuperreuse voorkom. [2]
Die radius hier bo is groter as wat sterevolusie voorspel en kan dus onbetroubaar wees[3]
Saturnus se wentelbaan 1 940 - 2 169 Aangedui vir grootteverwysing
Grootste sterre? ~1 500 Teoreties die limiet van stergroottes in die Melkweg [3]
RSGC1-F01 1 450[4] - 1 530[5] Geleë in die oop sterreswerm RSGC1.
VY Canis Majoris 1 420 ± 120 Is voorheen as die grootste bekende ster beskryf gebaseer op ’n radius van 1 800 - 2 100 sonradiusse.
CM Velorum 1 416 [6]
AH Scorpii 1 411 ± 124
RSGC1-F06 1 382 Geleë in die oop sterreswerm RSGC1. [5]
CD-26 5055 1 280 [6]
AS Cephei 1 263 [6]
RSGC1-F10 1 246 Geleë in die oop sterreswerm RSGC1. [5]
Westerlund 1-237
(Westerlund 1 BKS B)		 1 241 [7]
IRC-10414 ~1 200 [8]
V517 Monocerotis ~1 196 [6]
PZ Cassiopeiae 1 190 [3]
BC Cygni 1 187 'n Ouer studie met meer besonderhede gee 'n waarde van 1 081 - 1 375 vir die jaar 2000, en 1 303 - 1 553 vir die jaar 1900. [9]
MY Cephei 1 135 Ouer ramings was tot 2 440 sonradiusse, gebaseer op baie koeler temperature. [5]
RSGC1-F02 1 128 Geleë in die oop sterreswerm RSGC1. [5]
Jupiter se wentelbaan 1 114 - 1 115 Aangedui vir grootteverwysing
V766 Centauri Aa 1 110 'n Seldsame veranderlike geelsuperreus. [10]
RW Cygni 1 103 [11]
RSGC1-F04 1 100[4] - 1 500[5] Geleë in die oop sterreswerm RSGC1.
RT Carinae 1 090 [3]
V384 Persei 1 088 [12]
UU Persei 1 079 [6]
R Fornacis 1 078 [12]
V396 Centauri 1 070[3] - 1 145,31[13]
HD 126577 1 066 [6]
V1300 Aquilae (IRC-10529) 1 059 [14]
HaroChavira 1 1 058 [15]
V602 Carinae 1 050 [16]
WX Piscium 1 044 [14]
KU Andromedae (IRC +40004) 1 044 [14]
RSGC1-F11 1 032 Geleë in die oop sterreswerm RSGC1. [5]
KY Cygni 1 032[15] - 1 420[3]
RW Leonis Minoris 1 028 [14]
V346 Puppis 1 025 [12]
RSGC1-F13 1 017[5] - 1 430[4] Geleë in die oop sterreswerm RSGC1.
CK Carinae 1 013 - 1 060 [3]
KW Sagittarii 1 009 [17][18]
RSGC1-F07 1 006 Geleë in die oop sterreswerm RSGC1. [5]
V349 Carinae 1 002 [6]
Die volgende sterre met groottes onder 1 000 sonradiusse word aangedui ter vergelyking
RW Cephei 940 [19]
LL Pegasi 869 [20]
BI Cygni 851 - 1 240 [21][3]
UY Scuti 825[22] - 1 708[17] Die hoogste skatting vir UY Sct is hoër as wat volgens sterevolusie voorspel word. Die rede hiervoor is nie duidelik nie.[23]
Betelgeuse (α Orionis) 764[24] - 1 021[25] Tiende helderste ster in die naglug.
Antares A (α Scorpii) 680 Veertiende helderste ster in die naglug.[26] [27]
Mira A (ο Ceti) 541 [20]
Mars se wentelbaan 322 - 323 Aangedui vir grootteverwysing
Pistoolster (V4647 Sagittarii) 306 [28]
Rasalgethi A (α Herculis) 284 - 264 [29]
Aarde se wentelbaan (1 AE) 214 Aangedui vir grootteverwysing
Enif (ε Pegasi) 210,4 - 210,7 [30]
Deneb (α Cygni) 203 Agttiende helderste ster in die naglug.[26] [31]
Mercurius se wentelbaan 82,9 - 84,6 Aangedui vir grootteverwysing
Vega (α Lyrae) 2,726 - 2,418 Die vyfde helderste ster in die naglug. [32]
Son 1 Die grootste voorwerp in die Sonnestelsel.
Aangedui vir grootteverwysing
Grootste sterre in die Magellaanse Wolke
Sternaam Sonradius
(Son = 1) 		Sterrestelsel Notas Verwysings
WOH G64 1 540 Groot Magellaanse Wolk Die ster is omring deur 'n groot stofwolk. [33]
WOH S170 1 461 Groot Magellaanse Wolk [34]
HD 269551 1 439 Groot Magellaanse Wolk [34]
HV 12463 1 420 Groot Magellaanse Wolk [34]
W60 B90 (WOH S264) 1 390 Groot Magellaanse Wolk Nadere ondersoek is nodig om die helderheid en radius met groter sekerheid vas te stel. [35]
HV 888 1 374 Groot Magellaanse Wolk [34]
LMC 23095 1 280 Groot Magellaanse Wolk [34]
OGLE BRIGHT-LMC-LPV-52 1 275 Groot Magellaanse Wolk [34]
LMC 145013 1 234 Groot Magellaanse Wolk [34]
HV 5618 1 163 Groot Magellaanse Wolk [34]
LMC 25320 1 156 Groot Magellaanse Wolk [34]
SMC 18592 1 129 Groot Magellaanse Wolk [34]
SP77 21-12 1 103 Groot Magellaanse Wolk [34]
[W60] D44 1 063 Groot Magellaanse Wolk [34]
Grootste sterre in M31 en M33
Sternaam Sonradius
(Son = 1) 		Sterrestelsel Notas Verwysings
LGGS J013414.27+303417.7 1 479 Driehoeksterrestelsel (M33) Die radius van al die sterre in dié sterrestelsels is bereken volgens bolometriese helderheid en effektiewe temperatuur [34]
LGGS J004514.91+413735.0 1 324 Andromeda-sterrestelsel (M31) [34]
LGGS J004125.23+411208.9 1 302 Andromeda-sterrestelsel [34]
LGGS J013350.62+303230.3 1 283 Driehoeksterrestelsel [34]
LGGS J003951.33+405303.7 1 272 Andromeda-sterrestelsel [34]
LGGS J004124.80+411634.7 1 240 Andromeda-sterrestelsel [34]
LGGS J004035.08+404522.3 1 230 Andromeda-sterrestelsel [34]
LGGS J013409.63+303907.6 1 182 Driehoeksterrestelsel [34]
LGGS J013352.96+303816.0 1 182 Driehoeksterrestelsel [34]
LGGS J004047.22+404445.5 1 162 Andromeda-sterrestelsel [34]
LGGS J004428.48+415130.9 1 130 Andromeda-sterrestelsel [34]
LGGS J013335.90+303344.5 1 104 Driehoeksterrestelsel [34]
LGGS J013358.54+303419.9 1 103 Driehoeksterrestelsel [34]
LGGS J013336.64+303532.3 1 102 Driehoeksterrestelsel [34]
LGGS J013241.94+302047.5 1 083 Driehoeksterrestelsel [34]
LGGS J004059.50+404542.6 1 071 Andromeda-sterrestelsel [34]
LGGS J013430.75+303218.8 1 067 Driehoeksterrestelsel [34]
LGGS J013314.31+302952.9 1 067 Driehoeksterrestelsel [34]
LGGS J013412.27+305314.1 1 063 Driehoeksterrestelsel [34]
LGGS J013328.17+304741.5 1 063 Driehoeksterrestelsel [34]
LGGS J013233.77+302718.8 1 085 Driehoeksterrestelsel [34]
LGGS J013307.60+304259.0 1 081 Driehoeksterrestelsel [34]
LGGS J013305.48+303138.5 1 046 Driehoeksterrestelsel [34]
LGGS J013351.47+303640.3 1 034 Driehoeksterrestelsel [34]
LGGS J013303.54+303201.2 1 027 Driehoeksterrestelsel [34]
LGGS J004047.82+410936.4 1 010 Andromeda-sterrestelsel [34]
LGGS J013344.10+304425.1 1 007 Driehoeksterrestelsel [34]

Sien ook

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Verwysings

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  1. ↑ Ren, Yi; Jiang, Bi-Wei (Julie 2020). "On the Granulation and Irregular Variation of Red Supergiants". The Astrophysical Journal. 898 (1): 24. arXiv:2006.06605. Bibcode:2020ApJ...898...24R. doi:10.3847/1538-4357/ab9c17. ISSN 0004-637X.
  2. ↑ Fok, Thomas K. T; Nakashima, Jun-ichi; Yung, Bosco H. K; Hsia, Chih-Hao; Deguchi, Shuji (2012). "Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated with Massive Clusters". The Astrophysical Journal. 760 (1): 65. arXiv:1209.6427. Bibcode:2012ApJ...760...65F. doi:10.1088/0004-637X/760/1/65. S2CID 53393926.
  3. ↑ 3,0 3,1 3,2 3,3 3,4 3,5 3,6 3,7 Levesque, Emily M.; Massey, Philip; Olsen, K. A. G.; Plez, Bertrand; Josselin, Eric; Maeder, Andre; Meynet, Georges (Augustus 2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not As Cool As We Thought". The Astrophysical Journal. 628 (2): 973–985. arXiv:astro-ph/0504337. Bibcode:2005ApJ...628..973L. doi:10.1086/430901. ISSN 0004-637X.
  4. ↑ 4,0 4,1 4,2 Decin, Leen; Richards, Anita M. S.; Marchant, Pablo; Sana, Hugues (17 March 2023). "ALMA detection of CO rotational line emission in red supergiant stars of the massive young star cluster RSGC1 -- Determination of a new mass-loss rate prescription for red supergiants". [astro-ph.SR]. 
  5. ↑ 5,0 5,1 5,2 5,3 5,4 5,5 5,6 5,7 5,8 Humphreys, Roberta M.; Helmel, Greta; Jones, Terry J.; Gordon, Michael S. (Augustus 2020). "Exploring the Mass Loss Histories of the Red Supergiants". The Astronomical Journal (in Engels). 160 (3): 145. arXiv:2008.01108. Bibcode:2020AJ....160..145H. doi:10.3847/1538-3881/abab15.
  6. ↑ 6,0 6,1 6,2 6,3 6,4 6,5 6,6 Vallenari, A.; Brown, A. G. A.; Prusti, T. (13 Junie 2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics (in Engels). doi:10.1051/0004-6361/202243940. ISSN 0004-6361.
  7. ↑ Arévalo, Aura de Las Estrellas Ramírez (Julie 2018). The Red Supergiants in the Supermassive Stellar Cluster Westerlund 1 (in Engels). University of São Paulo. doi:10.11606/D.14.2019.tde-12092018-161841. {{cite book}}: Onbekende parameter |degree= geïgnoreer (hulp)
  8. ↑ Gvaramadze, V. V.; Menten, K. M.; Kniazev, A. Y.; Langer, N.; Mackey, J.; Kraus, A.; Meyer, D. M. -A.; Kamiński, T. (Januarie 2014). "IRC -10414: a bow-shock-producing red supergiant star". Monthly Notices of the Royal Astronomical Society. 437 (1): 843–856. arXiv:1310.2245. Bibcode:2014MNRAS.437..843G. doi:10.1093/mnras/stt1943. ISSN 0035-8711.
  9. ↑ Turner, David G.; Rohanizadegan, Mina; Berdnikov, Leonid N.; Pastukhova, Elena N. (November 2006). "The Long-Term Behavior of the Semiregular M Supergiant Variable BC Cygni". Publications of the Astronomical Society of the Pacific. 118 (849): 1533–1544. Bibcode:2006PASP..118.1533T. doi:10.1086/508905. ISSN 0004-6280.
  10. ↑ van Genderen, A. M.; Lobel, A.; Nieuwenhuijzen, H.; Henry, G. W.; De Jager, C.; Blown, E.; Di Scala, G.; Van Ballegoij, E. J. (2019). "Pulsations, eruptions, and evolution of four yellow hypergiants". Astronomy and Astrophysics. 631: A48. arXiv:1910.02460. Bibcode:2019A&A...631A..48V. doi:10.1051/0004-6361/201834358. S2CID 203836020.
  11. ↑ Norris, Ryan (27 Februarie 2021). "An Interferometric Imaging Survey of Red Supergiant Stars". The 20.5Th Cambridge Workshop on Cool Stars: 263. Bibcode:2021csss.confE.263N. doi:10.5281/zenodo.4567641.
  12. ↑ 12,0 12,1 12,2 Bergeat, J.; Chevallier, L. (Januarie 2005). "The mass loss of C-rich giants". Astronomy and Astrophysics. 429: 235–246. arXiv:astro-ph/0601366. Bibcode:2005A&A...429..235B. doi:10.1051/0004-6361:20041280.
  13. ↑ Stassun K.G.; et al. (Oktober 2019). "The revised TESS Input Catalog and Candidate Target List". The Astronomical Journal. 158 (4): 138. arXiv:1905.10694. Bibcode:2019AJ....158..138S. doi:10.3847/1538-3881/ab3467. S2CID 166227927.
  14. ↑ 14,0 14,1 14,2 14,3 Ramstedt, S.; Olofsson, H. (25 Mei 2014). "The 12CO/13CO ratio in AGB stars of different chemical type. Connection to the 12C/13C ratio and the evolution along the AGB". Astronomy and Astrophysics. 566: A145. arXiv:1405.6404. Bibcode:2014A&A...566A.145R. doi:10.1051/0004-6361/201423721. ISSN 0004-6361.
  15. ↑ 15,0 15,1 Comerón, F.; Djupvik, A. A.; Schneider, N.; Pasquali, A. (27 September 2020). "The historical record of massive star formation in Cygnus". Astronomy & Astrophysics. 2009: A62. arXiv:2009.12779. Bibcode:2020A&A...644A..62C. doi:10.1051/0004-6361/202039188.
  16. ↑ Arroyo-Torres, B.; Wittkowski, M.; Chiavassa, A.; Scholz, M.; Freytag, B.; Marcaide, J. M.; Hauschildt, P. H.; Wood, P. R.; Abellan, F. J. (Maart 2015). "What causes the large extensions of red supergiant atmospheres?. Comparisons of interferometric observations with 1D hydrostatic, 3D convection, and 1D pulsating model atmospheres". Astronomy and Astrophysics. 575: A50. arXiv:1501.01560. Bibcode:2015A&A...575A..50A. doi:10.1051/0004-6361/201425212. ISSN 0004-6361.
  17. ↑ 17,0 17,1 Arroyo-Torres, B.; Wittkowski, M.; Marcaide, J. M.; Hauschildt, P. H. (Junie 2013). "The atmospheric structure and fundamental parameters of the red supergiants AH Scorpii, UY Scuti, and KW Sagittarii". Astronomy and Astrophysics. 554: A76. arXiv:1305.6179. Bibcode:2013A&A...554A..76A. doi:10.1051/0004-6361/201220920. ISSN 0004-6361.
  18. ↑ Montargès, M.; et al. (5 Januarie 2023). "The VLT/SPHERE view of the ATOMIUM cool evolved star sample. I. Overview: Sample characterization through polarization analysis". Astronomy and Astrophysics. 671: A96. arXiv:2301.02081. Bibcode:2023A&A...671A..96M. doi:10.1051/0004-6361/202245398.
  19. ↑ Jones, Terry Jay; Shenoy, Dinesh; Humphreys, Roberta (Mei 2023). "The Recent Mass Loss History of the Hypergiant RW Cep". Research Notes of the American Astronomical Society. 7 (5): 92. Bibcode:2023RNAAS...7...92J. doi:10.3847/2515-5172/acd37f. ISSN 2515-5172.
  20. ↑ 20,0 20,1 De Beck, E.; Decin, L.; De Koter, A.; Justtanont, K.; Verhoelst, T.; Kemper, F.; Menten, K. M. (2010). "Probing the mass-loss history of AGB and red supergiant stars from CO rotational line profiles. II. CO line survey of evolved stars: Derivation of mass-loss rate formulae". Astronomy and Astrophysics. 523: A18. arXiv:1008.1083. Bibcode:2010A&A...523A..18D. doi:10.1051/0004-6361/200913771.
  21. ↑ Josselin, E.; Plez, B. (Julie 2007). "Atmospheric dynamics and the mass loss process in red supergiant stars". Astronomy and Astrophysics. 469 (2): 671–680. arXiv:0705.0266. Bibcode:2007A&A...469..671J. doi:10.1051/0004-6361:20066353. ISSN 0004-6361.
  22. ↑ Van Loon, J. Th.; Cioni, M.-R. L.; Zijlstra, A. A.; Loup, C. (2005). "An empirical formula for the mass-loss rates of dust-enshrouded red supergiants and oxygen-rich Asymptotic Giant Branch stars". Astronomy and Astrophysics. 438 (1): 273–289. arXiv:astro-ph/0504379. Bibcode:2005A&A...438..273V. doi:10.1051/0004-6361:20042555.
  23. ↑ Wittkowski, M.; Arroyo-Torres, B.; Marcaide, J. M.; Abellan, F. J.; Chiavassa, A.; Guirado, J. C. (Januarie 2017). "VLTI/AMBER spectro-interferometry of the late-type supergiants V766 Cen (=HR 5171 A), σ Oph, BM Sco, and HD 206859". Astronomy and Astrophysics. 597: A9. arXiv:1610.01927. Bibcode:2017A&A...597A...9W. doi:10.1051/0004-6361/201629349. ISSN 0004-6361.
  24. ↑ Joyce, Meridith; Leung, Shing-Chi; Molnár, László; Ireland, Michael; Kobayashi, Chiaki; Nomoto, Ken'ichi (Oktober 2020). "Standing on the Shoulders of Giants: New Mass and Distance Estimates for Betelgeuse through Combined Evolutionary, Asteroseismic, and Hydrodynamic Simulations with MESA". The Astrophysical Journal. 902 (1): 63. arXiv:2006.09837. Bibcode:2020ApJ...902...63J. doi:10.3847/1538-4357/abb8db. ISSN 0004-637X.
  25. ↑ Kravchenko, K.; Jorissen, A.; Van Eck, S.; Merle, T.; Chiavassa, A.; Paladini, C.; Freytag, B.; Plez, B.; Montargès, M.; Van Winckel, H. (1 April 2021). "Atmosphere of Betelgeuse before and during the Great Dimming event revealed by tomography". Astronomy & Astrophysics. 2104: arXiv:2104.08105. arXiv:2104.08105. Bibcode:2021A&A...650L..17K. doi:10.1051/0004-6361/202039801. S2CID 233289746.
  26. ↑ 26,0 26,1 Hoffleit, D.; Warren, W. H. Jr. (November 1995). "VizieR Online Data Catalog: Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991)". VizieR Online Data Catalog: V/50. Bibcode:1995yCat.5050....0H.
  27. ↑ Ohnaka, K.; Hofmann, K. -H.; Schertl, D.; Weigelt, G.; Baffa, C.; Chelli, A.; Petrov, R.; Robbe-Dubois, S. (Julie 2013). "High spectral resolution imaging of the dynamical atmosphere of the red supergiant Antares in the CO first overtone lines with VLTI/AMBER". Astronomy and Astrophysics. 555: A24. arXiv:1304.4800. Bibcode:2013A&A...555A..24O. doi:10.1051/0004-6361/201321063. ISSN 0004-6361.
  28. ↑ Najarro, Francisco; Figer, Don F.; Hillier, D. John; Geballe, T. R.; Kudritzki, Rolf P. (Februarie 2009). "Metallicity in the Galactic Center: The Quintuplet Cluster". The Astrophysical Journal. 691 (2): 1816–1827. arXiv:0809.3185. Bibcode:2009ApJ...691.1816N. doi:10.1088/0004-637X/691/2/1816. ISSN 0004-637X.
  29. ↑ Moravveji, Ehsan; Guinan, Edward F.; Khosroshahi, Habib; Wasatonic, Rick (Desember 2013). "The Age and Mass of the α Herculis Triple-star System from a MESA Grid of Rotating Stars with 1.3". The Astronomical Journal. 146 (6): 148. arXiv:1308.1632. Bibcode:2013AJ....146..148M. doi:10.1088/0004-6256/146/6/148. ISSN 0004-6256.
  30. ↑ Stock, S.; Reffert, S.; Quirrenbach, A. (Mei 2018). "VizieR Online Data Catalog: Stellar parameters of 372 giant stars (Stock+, 2018)". VizieR On-line Data Catalog. 361 (33): 600. Bibcode:2018yCat..36160033S.
  31. ↑ Schiller, F.; Przybilla, N. (Maart 2008). "Quantitative spectroscopy of Deneb". Astronomy and Astrophysics. 479 (3): 849–858. arXiv:0712.0040. Bibcode:2008A&A...479..849S. doi:10.1051/0004-6361:20078590. ISSN 0004-6361.
  32. ↑ Monnier, J. D.; Che, Xiao; Zhao, Ming; Ekström, S.; Maestro, V.; Aufdenberg, Jason; Baron, F.; Georgy, C.; Kraus, S.; McAlister, H.; Pedretti, E. (Desember 2012). "Resolving Vega and the Inclination Controversy with CHARA/MIRC". The Astrophysical Journal. 761 (1): L3. arXiv:1211.6055. Bibcode:2012ApJ...761L...3M. doi:10.1088/2041-8205/761/1/L3. ISSN 0004-637X.
  33. ↑ Levesque, Emily M.; Massey, Philip; Plez, Bertrand; Olsen, Knut A. G. (2009). "The Physical Properties of the Red Supergiant WOH G64: The Largest Star Known?". The Astronomical Journal. 137 (6): 4744. arXiv:0903.2260. Bibcode:2009AJ....137.4744L. doi:10.1088/0004-6256/137/6/4744.
  34. ↑ 34,00 34,01 34,02 34,03 34,04 34,05 34,06 34,07 34,08 34,09 34,10 34,11 34,12 34,13 34,14 34,15 34,16 34,17 34,18 34,19 34,20 34,21 34,22 34,23 34,24 34,25 34,26 34,27 34,28 34,29 34,30 34,31 34,32 34,33 34,34 34,35 34,36 34,37 34,38 Massey, Philip; Neugent, Kathryn F.; Ekstrom, Sylvia; Georgy, Cyril; Georges, Meynet (2023). "The Time-Averaged Mass-Loss Rates of Red Supergiants As Revealed by their Luminosity Functions in M31 and M33". The Astrophysical Journal. 942 (2): 35. arXiv:2211.14147. Bibcode:2023ApJ...942...69M. doi:10.3847/1538-4357/aca665.
  35. ↑ de Wit, S.; Bonanos, A.Z.; Tramper, F.; Yang, M.; Maravelias, G.; Boutsia, K.; Britavskiy, N.; Zapartas, E. (2023). "Properties of luminous red supergiant stars in the Magellanic Clouds". Astronomy and Astrophysics. 669: 17. arXiv:2209.11239. Bibcode:2023A&A...669A..86D. doi:10.1051/0004-6361/202243394.

Eksterne skakels

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